Note: Descriptions are shown in the official language in which they were submitted.
WO 2023/047263
PCT/IB2022/058835
1
OPTICAL BEAMFORMING AND INTERFEROMETRY USING DIGITAL
SOURCE MODULATION
FIELD OF THE INVENTION
[0001] The present disclosure relates generally to radio
astronomy digital signal
processing and timing. More particularly, examples of the disclosure relate to
a system and
method for optical beamforming and interferometry using digital source
modulation.
BACKGROUND OF THE DISCLOSURE
[0002] Large mirrors and adaptive optics using wavetront
sensing and deformable
mirrors, and optical interferometry with complex and expensive mirror-mirror
(i.e. "baseline-
based") sidereal delay tracking, are known for high spatial resolution
applications such as
optical astronomy and satellite-to-Earth (downlink) and Earth-to-satellite
(uplink) free-space
optical communications ("sat-comm.')
[0003] However, single large optical mirrors are expensive
and subject to a
fundamental limit due to gravitational bending effects of large, massive,
mechanical
structures. Additionally, atmospheric turbulence across the aperture of an
optical mirror
requires the use of electro-mechanical adaptive optics. The number of mirrors
in an optical
interferometer is limited due to baseline-based sidereal delay tracking. The
size of an optical
interferometer array (i.e. the "array aperture") is limited due to the
requirement for precision
optics required for coordinating all of the mirrors. Sat-comm is subject to
complexity/limitations of downlink and uplink adaptive optics and cost and
size of mirrors.
[0004] Any discussion of problems provided in this section
has been included in this
disclosure solely for the purposes of providing a background for the present
invention, and
should not be taken as an admission that any or all of the discussion was
known at the time
the invention was made.
BRIEF DESCRIPTION OF THE DRAWING FIGURES
[0005] The subject matter of the present disclosure is
particularly pointed out and
distinctly claimed in the concluding portion of the specification. A more
complete
understanding of the present disclosure, however, may best be obtained by
referring to the
detailed description and claims when considered in connection with the drawing
figures,
wherein like numerals denote like elements and wherein:
[0006] FIG. 1 illustrates a system for optical beamforming
and interferometry using
digital source modulation, in accordance with exemplary embodiments of the
disclosure.
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/IB2022/058835
2
[0007] FIG. 2 shows sub-aperture calibration using digital
source modulation, in
accordance with exemplary embodiments of the disclosure.
[0008] FIG. 3 shows an exemplary station reference clock and
DSM message decoder
of the system depicted in FIG. 1.
[0009] FIG. 4 shows an exemplary per-sub-aperture PID servo
of the system depicted
in FIG. 1.
[0010] FIG. 5 shows an exemplary DAC/ADC block of the per-sub-
aperture PID servo
of the system depicted in FIG. 4.
[0011] FIG. 6 shows a system for station beam offset for
astronomical applications, in
accordance with exemplary embodiments of the disclosure.
[0012] FIG. 7 illustrates a system for optical astronomy
aperture synthesis
(interferometry) , in accordance with exemplary embodiments of the disclosure.
[0013] FIG. 8 shows an exemplary lag correlator of the system
depicted in FIG. 7.
[0014] It will be appreciated that elements in the figures
are illustrated for simplicity
and clarity and have not necessarily been drawn to scale. For example, the
dimensions of
some of the elements in the figures may be exaggerated relative to other
elements to help to
improve understanding of illustrated embodiments of the present disclosure.
DETAILED DESCRIPTION OF EXEMPLARY EMBODIMENTS
[0015] As discussed below, a system and method are provided
for optical
beamforming and interferometry using digital source modulation. In one aspect,
a digitally-
modulated calibration signal, referred herein to as "Digital Source
Modulation'. (DSM), is
included in the optical target source, for use by receiving minors and
equipment to
continuously lock onto, track, and remove atmospheric and instrumental
temporal distortion
effects. By using this digitally-modulated calibration signal throughout the
optical signal chain
any variations that both it and the science/payload signal undergo can be
removed, leading to
lower cost optical minors and optical interferometers, as well as allowing for
larger optical
apertures.
[0016] For sat-comm, the DSM signal can be one optical colour
of a Dense
Wavelength Division Multiplexing (DWDM) signal, with the other colours of the
DWDM
signal being high data rate communications "payload".
[0017] For astronomy, the DSM signal can be a laser signal
transmitted by one or more
optical "Satellite Guide Stars" (SOS), each with an orbit that allows a
sufficient period of time
close to the science target to be used as a calibrator.
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
3
[0018] For both sat-comm and astronomy, the DSM calibration
signal can be ON/OFF
modulation of an optical monochromatic carrier, wherein the modulation
contains signaling
to allow synchronized production, at each receiving element, of a high-purity
complex digital
monochromatic signal (i.e. "tone"), referred to herein as a "tracer." Since
the DSM calibration
signal comes from a source that is common to all receiving elements, and
follows the identical
or nearly identical optical path as the science or payload signal, any delay
differences in the
DSM at each receiving element, which are removed before further beamforming
(summing)
and/or interferometer (multiply-accumulate) operations, also therefore apply
to the science or
payload signal.
[0019] Since both the DSM optical carrier and encoded digital
signal (tracer) are
monochromatic, the DSM fundamentally forms the highest SNR (signal-to-noise
ratio)
calibrator signal possible since all calibration signal power is concentrated
into a very narrow
bandwidth.
[0020] According to an aspect of this specification, a system
is provided for optical
hearnforming and interferometry using digital source modulation, comprising a
plurality of
sub-apertures, including a reference sub-aperture, for receiving and
transmitting a digital
source modulation (DSM) signal and payload/science signal via respective
optical
waveguides, wherein temporal variations in the optical waveguides are
indiscernible from
atmospheric variations; a plurality of per-sub-aperture PID servos for
receiving the DSM
signal and payload/science signal from the optical waveguides and performing
delay
correction/compensation operations to remove atmospheric and temporal optical
waveguide
variations; a station reference clock and DSM (tracer) message decoder for
receiving the DSM
signal from the reference sub-aperture and outputting reference clock signals
to the plurality
of per-sub-aperture PID servos; an optical beamformer/summer for summing the
optical
payload and DSM signals from which atmospheric and temporal optical waveguide
variations
have been removed by the plurality of per-sub-aperture PID servos; and a
calibration block
for receiving the summed optical payload and DSM signals and generating and
transmitting
coherency calibration signals to the plurality of per-sub-aperture PID servos
for establishing
coherence between the optical payload and DSM signals output from the
plurality of per-sub-
aperture PID servos.
[0021] According to an aspect of this specification, a method
of establishing coherence
of an optical payload and DSM signals from a plurality of sub-apertures, from
which
atmospheric and temporal optical waveguide variations have been removed by a
plurality of
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
4
per-sub-aperture PID servos, comprising: opening a light path of a reference
sub-aperture; and
aligning the optical payload and DSM signals; and opening the light paths for
all sub-apertures
to obtain a beamformed sum of the DSM colour and payload colours.
[0022] Turning to FIG. 1, a system 100 is shown for optical
beamforming and
interferometry using digital source modulation, in accordance with exemplary
embodiments
of the disclosure. A plurality of "sub-apertures" are provided in the form of
mirrors (or sub-
parts of a larger mirror) 100i...100m, 100õ,Ref, each of a size (Ro) such that
the PSF (point-
spread function) of the received DSM signal and payload/science signal is at
its diffraction
limit (note that there must be sufficient DSM signal power and sensitivity for
each sub-
aperture to independently lock onto the DSM signal). The DSM signal and
payload/science
signal may optionally be amplified by a low noise amplifier (not shown) for
amplifying the
total optical signal before processing by associated per-sub-aperture PID
servos 1101...110m,
110.Ref, where "P" refers to proportional gain, "I" refers to integral gain,
and "D" refers to
derivative gain. Within each per-sub-aperture PID servo 1101...110m, 110mRef,
delay
correction/compensation operations are performed to remove atmospheric and
temporal
optical waveguide variations.
[0023] An optical beamformer/summer 120 adds the optical
payload and DSM signal
corrected for the atmosphere by the PID servos 110i...110m, 110mRef. However,
differential
delays in the optics, electronics, and optical paths of the PID servos
110i...110m, 110,õRef are
such that the outputs of the PM servos 110i... 110m, 110mRef do not add
coherently at the
optical wavelength. Thus, calibration block 130 establishes coherence. With
the light path of
the Reference sub-aperture 100mRef open, the light path for each sub-aperture
1001...100m is
opened sequentially thereby feeding the DSM signal/colour from
beamformer/summer 120
into an optical power detector 130, which in embodiments can be a photo
detector and ADC.
The tracer DDS phase ("coherency_cal" ) of the sub-aperture being calibrated
is then adjusted
in a per-sub-aperture fine coherency calibrator 140 until maximum optical
power is detected.
As shown in FIG. 2, maximum power is obtained when the optical carrier and DSM
symbols
are perfectly aligned. In embodiments, a sensitive peak-finding algorithm can
be provided
that combines a low-rate linear step/sweep and low-amplitude (e.g. few MHz) of
sinusoidal
modulation of the coherency_cal signal. Then, for each step, the few MHz
modulation signal
can be cross-correlated and integrated with the ADC output of optical power
detector 130 until
a peak in the Fourier Transform of the cross-correlation function (of the few
MHz modulation)
is found. It is contemplated that calibration may be possible without opening
the optical light
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
paths to the sub-apertures, by using a different modulation frequency
simultaneously for each
sub-aperture 100i...100m and searching for the peak in the cross-correlation
function for each.
[0024] The coherency_cal signal is a phase offset into a
tracer direct digital
synthesizer, DDS 480, that offsets (i.e. biases) an optical delay 400,
discussed below with
reference to FIGS. 4 and 5, by a corresponding amount. A coherency_cal
resolution of a
fraction of an optical wavelength is required; for example for a 32-bit tracer
DDS at a tracer
frequency of 100 MHz, 1/(100 MHz x 2^32) ¨= le-18 sec of delay resolution can
be obtained,
depending on the transfer function of optical delay 400. For example, at an
optical wavelength
of 2.=1500 nm, le-18 sec corresponds to an optical phase resolution of ch. x
le-18 sec, or
¨0.072 degrees.
[0025] After coherency calibration, the optical signals'
output from PID servos
110i...110m, 110.Rer must be differentially (i.e. every sub-aperture relative
to all others)
temporally stable in delay to a fraction of an optical wavelength. In each PID
servo
110i...110m, 1101-i-aer this can be accomplished by length matching and
temperature stabilizing
all critical electrical paths. In practice, periodic coherency calibration may
be required to
ensure continued coherence.
[0026] An optional low noise amplifier (LNA) 150 may be
provided, although not
required for sat-comm applications since the coherent beamformed signal is
ready for payload
extraction without it, whereas for astronomy aperture synthesis, LNA 150 may
be required to
drive additional optical paths, as discussed with reference to FIG. 7.
[0027] Once the coherency calibration procedure discussed
above is performed for
every sub-aperture, the light paths for all sub-aperture 1001...1001\4,
100,õRef are opened to
obtain a final beamformed sum of the DSM colour and payload colours. This
summed signal
may then be subject to further payload extraction and processing (not shown),
with the DSM
signal either discarded or used for optical link performance monitoring.
[0028] Station reference clock and DSM (tracer) message
decoder 160 receives the
DSM colour output from reference sub-aperture 100r,,Ref, and outputs reference
clock signals
st_ref clk and st_ref clk_adc, to the PID servos 1101...110m, 110.R.r.
[0029] An exemplary station reference clock and DSM message
decoder 160 is shown
in FIG. 3. Optical-to-electrical (photo) detector 300 extracts the DSM colour
from reference
sub-aperture 100,õRef and converts it to an electrical (voltage) on/off
signal. Clock-data-
recovery (CDR) PLL and frequency synthesizer 310 extracts a clock from the DSM
signal for
decoding by DSM decoder 320 as tr_phase + sync and is written to a FIFO 330
for use in the
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
6
st_ref_clock domain to periodically load/initialize the init_accum input of
each PID servo
1101...110m, 11011,Rer , as discussed with reference to FIG. 4. The
st_ref_clock is a "digital
quality" clock used for discrete digital operations of the PID servos
1101...110m, 1101i,Ref; its
actual jitter has no impact on servo performance, other than meeting digital
circuitry timing
needs. However, the (differential) jitter performance of st_rel clock_adc at
each DSM carrier
tone ADC 450 (FIG. 4) is important as it determines PID servo tracking
performance in terms
of loop bandwidth and optical wavelength operation, since it affects phase
noise in the output
of DSM carrier tone ADC 450. Typically st_ref clock_adc needs to be better
than -50 fsec
RMS (differential) at each ADC clock input, depending on loop bandwidth and
optical
wavelength.
[0030] Jitter cleaner 340 cleans the raw output from CDR PLL
frequency synthesizer
310 for use as the station reference clocks, st_ref_clock and
st_ref_clock_adc, both the same
frequency and phase, but with different qualities as described above. Jitter
cleaner 340 can be
a null function, or may cut off atmospheric phase variations of the DSM signal
at a defined
cutoff frequency.
[0031] Turning now to FIG. 4, additional details of each PID
servo 1101...110m,
110mRef are shown. Optical delay 400 is a pure single-axis optical delay,
driven by an optical
Delay adjust signal from low pass filter (LPF) 410, whose dynamic temporal and
range
response must be sufficient for atmospheric delay compensation, relative to
the st_ref_clock
produced by the jitter cleaner 340. Also, its transfer function (i.e. optical
delay adjust voltage-
to-delay transfer function) need not be precisely known since the PlD servo
loop compensates
for it.
[0032] A copy of the DSM signal colour is fed through an
optical-to-electrical
demodulator 420 (i.e. ON/OFF photo detector) into a DAC/ADC block 430 of the
per-sub-
aperture PID servo, comprising a DSM carrier tone DAC 440 and DSM carrier tone
ADC 450.
A DSM-derived monochromatic tone ("carrier tone") is captured within the
DAC/ADC block
430 into the common digital clock domain st_ref_clock. The performance of
block 430, in
capturing the DSM carrier tone without systematic phase noise effects that are
not due to the
atmosphere, determines PID servo bandwidth performance (i.e. atmospheric
correction speed)
and the useful optical wavelength. FIG. 5 provides additional details of block
diagram of
block 430 and its operation, although other methods may be used to accomplish
the same
result.
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
7
[0033] In FIG. 5, the DSM signal, which is mostly a digital
square wave but with
periodic DSM message content (i.e. tracer), is buffered/amplified at 500 and
filtered via LPF
510 to yield only the DSM signal fundamental frequency to, which is then
digitized into the
st_ref clock(_adc) clock domain. As such, buffer/amplifier 500 and LPF 510
provide the
functionality of DSM carrier tone DAC 440. DSM messages result in an increase
in spectral
content around f_o, resulting in a very short and inconsequential reduction in
station
beamforming coherence, which can be outside the PID servo loop bandwidth. It
will be
appreciated that the functionality illustrated in FIG. 5 may be accomplished
by other methods
and circuitry.
[0034] The output of ADC 450 is a "real" digitized sinusoid
of the DSM carrier tone
and therefore carries no phase information except that all sub-aperture
outputs are at similar
phases within ¨7-c/8 of each other so there is no phase ambiguity when it
comes to "coherency
calibration", as discussed further below. In order to provide phase for
calibration,
beamforming, and station beam steering, the "real" digitized sinusoid of the
DSM carrier tone
must be turned into a complex signal by an I/Q mixer 460, with a complex
sinusoidal input
whose phase and frequency is extracted from the periodically-transmitted DSM
message
(tracer), which is generated by DDS 350 in station reference clock and DSM
message decoder
160 (FIG. 3). The result of this operation is complex, with tones in the
complex frequency
domain at the DSM carrier tone +/- the l/Q mixer frequency, with one (i.e.
generated by DDS
350) at the DSM tracer frequency, and another at a higher frequency, which
must be digitally
filtered out via digital LPF 470, before a CMAC it detector 490 (where
CMAC,Complex
Multiply-Accumulate). Alternatively, the complex output of complex multiplier
in detector
490 can be digitally filtered before accumulation. By making the unwanted
complex image a
substantially different frequency than the wanted image, the digital LPF
filter 470 can be
optimized in terms of hardware and latency. For example, if the DSM carrier
tone f o is 150
MHz and the tracer produced by DDS 480 is 100 MHz, then the I/Q mixer
frequency is 50
MHz, with one output at 100 MHz and one at -200 MHz, with the latter filtered
by the digital
LPF 470.
[0035] A digital phase ramp output from tracer DDS 480 is
converted to digital sine
and cosine via a LookUp Table (LUT 480B), before use in the CMAC detector 490,
where the
phase and frequency is the same for each sub-aperture (and station): for the
former, periodic
messages encoded in the DSM signal (i.e.DSM tracer messages) update its phase
so that all
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
8
sub-apertures and stations are aligned, with only the atmosphere across them
different; for the
latter, each tracer DDS 480 operates with the same system-wide phase
increment.
[0036] Inputs to the phase offset ("poff') of the tracer DDS
480 include the
coherency_cal signal and the beam_offset, which are both digital values that
are summed at
495. The coherency_cal signal comes from the per-sub-aperture calibration
process discussed
above in connection with the per-sub-aperture fine coherency calibrator 140.
The beam_offset
is set differently for each sub-aperture (i.e. "delay-and-sum" beam steering)
to steer the station
beam to the payload/science source, if needed, as discussed below with
reference to FIG. 6.
Both the coherency_cal signal and the beam_offset signal bias the optical
delay 400 to
achieve station beam coherence, but steered in the direction of the
science/payload target. For
sat-comm applications, typically beam_offset=0 since the DSM signal and the
optical payload
are transmitted from the same source, whereas for optical astronomy
beam_offse03 since the
science target source is not the DSM source.
[0037] The output of DDS 480 and LUT 480B is connected to a
PID 498, for
calculating the PID coefficients, accumulating the result and outputting to a
LPF 410 which
filters out any phase variations and phase noise that are on timescales faster
than the
atmosphere correction time, Tau_atm, to produce an "Optical Delay adjust-
signal. LPF 410
may be digital or analogue, or be inherent in the frequency response of the
Optical Delay.
[0038] The Optical Delay adjust signal drives the optical
delay 400, thereby
completing the per-sub-aperture PID servo loop 1101...110m, 110mRef, such that
the loop tracks
and removes the effects of atmospheric fluctuations on the DSM signal and in
so doing, the
optical payload signals as well.
[0039] Turning now to FIG. 6, station beam offset is
depicted, which is normally only
required for astronomy applications. The DSM signal from a satellite guide
star (SGS) 600,
is offset from the astronomy science source 610. With a non-zero beam_offset,
coherence is
established and maintained on the DSM signal, whilst the actual station beam
is pointed to the
science source 610. The degree of offset determines science source coherence,
since its
photons traverse a different atmosphere than the DSM signal.
[0040] For optical astronomy aperture synthesis
(interferometry), as shown in FIG. 7,
each station 7001...700ref...700N corresponds to a system 100 as shown in FIG.
1, wherein the
output of each station comprises a beamformed sum of the DSM colour and
payload colours
for each station, with each wavefront-corrected to each st_ref_clk
independently, and with
small unknown delay offsets that can be calibrated by correlating on an
astronomical
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
9
calibrator, as discussed below, with delay adjusted to obtain fringes at 0-
delay. Reference
station 700rer is preferably positioned near the array phase center.
[0041] Blocks 7101...710rd...710N are similar to per-sub-
aperture PID servos 110 in
Fig. 4, except that the optical delay 400 contains delay to perform final
atmospheric delay
compensation of each station 7001... 700N to the smoothed central_ref clk +
tracer signal from
reference station 700,cf, and the full range of wavefront delay compensation
required as the
astronomical science source tracks at the sidereal rate across the sky. The
latter can be
implemented, for example, with a binary sequence of fiber lengths (e.g. on
spools), with
lengths switched in and out such that the error in total optical delay is
sufficiently small,
typically ¨10 degrees RMS at the optical wavelength. It should be noted that
since the DSM
and science signal go through the same delay path, each PID servo block
7101...710ier...710N
compensates for any temporal variations or absolute uncertainties, and the
delay can be
implemented, relative to a common geographical point (known at the array
"phase-center",
typically a virtual physical point near the geometric center of the array), on
a per-station basis,
resulting in a significant improvement over the prior art per-baseline (i.e.
antenna pair)
requirement in optical interferometry. In each PID servo block
710i...710ra...710N, the optical
delay has a much larger range (i.e. fiber cable segments + short-range
dynamic) and may be
temporally varying. Only the st_ref clk to central_ref clk phase wander and
delay tracking
is required to be accommodated.
[0042] A wavefront geometrical delay model is applied to each
PID servo block
7101 ...710,f...710N via per-station interferometer delay model (t) generator
720, for applying
a model of the delay phase_offset (delay)(t) within each PID servo block
7101...710ref...710N.
Since the delay range that must be accommodated, many cycles of the DSM tracer
frequency
are required, for example 100 MHz, introducing a phase ambiguity problem. To
deal with
this, the DSM message contains one or more lower tracer frequency phase
"init_accum"
messages, for one or more lower tracer frequency DDSs (not shown), used to
resolve this issue
with the PID servo block 710 closing the loop on all of these frequencies
simultaneously, and
a "beam_offser developed for each one, depending on the delay range it can
capture without
phase ambiguity. For example, if a 1 kHz ultra-low-frequency tracer is used,
with a period
T_lf tracer of 1 msec, it can be used to resolve the phase ambiguity up to ¨+/-
T_lf tracer/8 Or
125 microseconds. Here. the 1 kHz servo phase accuracy need only be such that
it is within
the high frequency tracer (e.g. 100 MHz) phase ambiguity "capture range." For
this low-
frequency, low-accuracy tracer, all-digital processing may be employed instead
of
analogue/digital processing as depicted in Fig. 5, wherein the DAC 440
comprises a DDS and
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
its output digital phase ramp is captured into the st_ref clock domain using
all-digital clock-
domain crossing methods.
[0043] The output of each PID servo block
7101...710,er...710N is a DSM and science
signal that is fully atmosphere-compensated and wavefront-delayed and ready
for cross-
correlation in an optical cross-correlation spectrometer 730. These signals
need to be stable,
but only inasmuch as any differential variation in them can be removed by
optical cross-
correlation spectrometer 730 using astronomical point-source calibration. The
optical cross-
correlation spectrometer 730 produces visibilities for each pair of stations
(i.e. "baseline") in
the array. Since the (wavefront) geometrical delay model applied to each PID
servo block
710i...710,f...710N via per-station inferometer delay model (t) generator 720
is merely a model
of the delay, and not the actual delay at the time of observing, the cross-
correlation function
must be adequately sampled in relative delay so that any residual (i.e.
difference between the
actual delay and the model) can be captured and corrected during visibility
(image) processing.
Thus, the optical cross-correlation spectrometer 730 must be able to capture
relative phase and
delay information between each pair of stations being processed.
[0044] Details of an exemplary optical cross-correlation
spectrometer 730 are shown
in FIG. 8, in the form of a "lag" correlator, as is known in the art, having a
plurality of optical-
optical multipliers 800 and delays 900, where delay= A /2. Input signals Xin
and Yin are
received from the two stations (X and Y) being cross-correlated such that
optical-optical
multiplier 800 produce an output that is the beat-difference-frequency of Xin
and Yin, in the
form of a voltage ranging from DC to up to ¨1 kHz (depending on the required
image field of
view), typically digitized with an ADC of sufficient precision (not shown),
and then digitally
accumulated for a prescribed period of time. Although a lag correlator is
shown in FIG. 8, it
is contemplated that other methods for a real cross-correlation to produce
complex visibilities
may be used.
[0045] The Fourier-transform of these accumulated lag points
is the complex cross-
power spectrum of the two stations being cross-correlated, with the number of
unique
frequency points being 1/2 the number of lags. A delay residual appears as a
phase-slope in the
cross-power spectrum, which can be periodically measured on a continuum
astronomical
source calibrator, and applied to the astronomical science source during image
processing,
which is a method well-established in the radio astronomy literature.
[0046] The DSM signal is effectively a narrow-band
interference (i.e. "RFI") signal
that forms a peak in the cross-correlation spectrum, suppressed somewhat
proportional to the
CA 03232526 2024- 3- 20
WO 2023/047263
PCT/1B2022/058835
11
geographical separation of the two stations X and Y and the offset of the SGS
600 from the
astronomical science source. In some embodiments, the signal may be notch-
filtered out of
the total optical signal before correlation which, as is known, produces a
spectral hole in the
science source spectrum.
[0047] The description of exemplary embodiments of the
present disclosure provided
below is merely exemplary and is intended for purposes of illustration only;
the following
description is not intended to limit the scope of the invention disclosed
herein. Moreover,
recitation of multiple embodiments having stated features is not intended to
exclude other
embodiments having additional features or other embodiments incorporating
different
combinations of the stated features.
[0048] The present invention has been described above with
reference to a number of
exemplary embodiments and examples. It should be appreciated that the
particular
embodiments shown and described herein are illustrative of the invention and
its best mode
and are not intended to limit in any way the scope of the invention as set
forth in the claims.
The features of the various embodiments may stand alone or he combined in any
combination.
Further, unless otherwise noted, various illustrated steps of a method can be
performed
sequentially or at the same time, and not necessarily be performed in the
order illustrated. It
will be recognized that changes and modifications may be made to the exemplary
embodiments without departing from the scope of the present invention. These
and other
changes or modifications are intended to be included within the scope of the
present invention,
as expressed in the following claims.
CA 03232526 2024- 3- 20
